The VFD potential U (σf) — derived from Coleman–Weinberg one-loop corrections and holographic entropy — yields a vacuum energy density V (σ₀) = λₑff/36 ≈ 2. 2×10⁻¹⁵ GeV⁴, which exceeds the observed cosmological constant Λₒbs ≈ 2. 9×10⁻⁴⁷ GeV⁴ by 32 orders of magnitude. The holographic screening factor κ = (lP/RH) ^ (1/3) ≈ 4. 9×10⁻²¹ has already removed 88 of the original 120 orders; the residual gap is localised in the holographic exponent n = 1/3. This paper attacks the 32-order gap directly. We compute the exact exponent nᵣeq ≈ 0. 848 that would close the gap and analyse its physical meaning as a shift in the holographic entropy counting from area-to-volume (2/3) toward an entanglement-dominated regime (≈5/3). The Cohen–Kaplan–Nelson UV–IR bound is shown to reproduce κ parametrically but not to fix n. Renormalisation-group running of the supertrace STr (μ) from the top-quark mass to the Hubble scale is computed threshold by threshold; STr decouples stepwise and approaches zero below the electron mass, but the running alone is insufficient to close the gap. Sub-leading holographic corrections (logarithmic Ryu–Takayanagi terms) contribute δn ~ 1/ln (RH/lP) ~ 1/140 — also insufficient in isolation. A holographic renormalisation group (HRG) framework, in which the exponent n (μ) runs from 1/3 in the UV to a larger IR value, is identified as the most promising structural pathway. A combined analysis in the (n, STr) plane maps the contour Λₒbs and shows that modest shifts in both parameters — n → 0. 6 combined with |STr| → 10⁻⁶ GeV⁴ — suffice without fine-tuning. All modifications are checked against frozen-field, BKT stability, and Eöt-Wash constraints; none are violated. The 32-order gap is thus localisable, decomposable, and constrainable — a qualitative advance over the unconstrained 10¹²⁰ of standard QFT.
Daniel Leonforte (Mon,) studied this question.